The Atmospheric Chemistry Experiment Fourier Transform Spectrometer (ACE-FTS) is the main instrument on-board the SCISAT-1 satellite, a mission mainly supported by the Canadian Space Agency [1]. It is in Low- Earth Orbit at an altitude of 650 km with an inclination of 74E. Its data has been used to track the vertical profile of more than 30 atmospheric species in the high troposphere and in the stratosphere with the main goal of providing crucial information for the comprehension of chemical and physical processes controlling the ozone life cycle. These atmospheric species are detected using high-resolution (0.02 cm-1) spectra in the 750-4400 cm-1 spectral region. This leads to more than 170 000 spectral channels being acquired in the IR every two seconds. It also measures aerosols and clouds to reduce the uncertainty in their effects on the global energy balance. It is currently the only instrument providing such in-orbit high resolution measurements of the atmospheric chemistry and is often used by international scientists as a unique data set for climate understanding.
The satellite is in operation since 2003, exceeding its initially planned lifetime of 2 years by more than a factor of 5. Given its success, its usefulness and the uniqueness of the data it provides, the Canadian Space Agency has founded the development of technologies enabling the second generation of ACE-FTS instruments through the High Vertical Resolution Measurement (HVRM) project but is still waiting for the funding for a mission.
This project addresses three major improvements over the ACE-FTS. The first one aims at improving the vertical instantaneous field-of-view (iFoV) from 4.0 km to 1.5 km without affecting the SNR and temporal precision. The second aims at providing precise knowledge on the tangent height of the limb observation from an external method instead of that used in SCISAT-1 where the altitude is typically inferred from the monotonic CO2 concentration seen in the spectra. The last item pertains to reaching lower altitude down to 5 km for the retrieved gas species, an altitude at which the spectra are very crowded in terms of absorption. These objectives are attained through a series of modification in the optical train such as the inclusion of a field converter and a series of dedicated real-time and post-acquisition algorithms processing the Sun images as it hides behind the Earth. This paper presents the concepts, the prototypes that were made, their tests and the results obtained in this Technology Readiness Level (TRL) improvement project.
Interferometers are devices meant to create an interference pattern between photons emitted from a given target of interest. In most cases, this interference pattern must be scanned over time or space to reveal useful information about the target (ex.: radiance spectra or a star diameter). This scanning is typically achieved by moving mirrors at a precision a few orders of magnitude smaller than the wavelength under study. This sometimes leads to mechanism requirements of especially high dynamic range equivalent to 30 bits or more (ex. Sub-nanometer precision over stoke of tens of cms for spectroscopy or tens of meters for astronomical spatial interferometry). On top of this mechanical challenge, the servo control of the mirror position involves obtaining relative distance measurement between distant optical elements with similar if not better dynamic range. The feedback information for such servo-control loop is usually the optical path difference (OPD) measured with a metrology laser beam injected in the interferometer. Over the years since the establishement of the Fourier Transform Spectrometers (FTS) in the 60’s as a standard spectroscopic tools, many different approaches have been used to accomplish this task. When it comes to space however, not all approaches are successful. The design challenge can be viewed as analogous to that of scene scanning modules with the exception that the sensitivity and precision are much finer. These mechanisms must move freely to allow fine corrections while remaining stiff to reject external perturbations with frequencies outside of the servo control system reach. Space also brings the additional challenges of implementing as much redundancy as possible and offering protection during launch for these sub-systems viewed as critical single point failures of the payloads they serve.
GOSAT-2 is the successor of the Greenhouse gases Observing SATellite (GOSAT, "IBUKI") launched in 2009 by Japan Aerospace Exploration Agency (JAXA). GOSAT-2 will continue and enhance space borne measurements of greenhouse gases started by GOSAT and monitor the impacts of climate change and human activities on the carbon cycle. It will also contribute to climate science and climate change related policies. The GOSAT-2 spacecraft will carry two earth observation instruments: FTS-2, the second generation of the TANSO-FTS and CAI-2, a Cloud and Aerosol Imager. Mitsubishi Electric Corporation is the prime contractor of GOSAT-2. Harris is the subcontractor of the spectrometer. ABB, who successfully designed, manufactured, and delivered the interferometer for the TANSO-FTS instrument for GOSAT, is currently delivering the modulator for the FTS-2 instrument to Mitsubishi Electric Corporation. Built on the TANSO-FTS heritage, FTS-2 is a thermal and near infrared sensor for carbon observation based on a Fourier transform spectrometer featuring larger optical throughput than TANSO-FTS. This paper presents an overview of the design of the FTS-2 interferometer as well as key qualification and performance verification activities conducted on the interferometer flight model.
Spectrally resolved infrared (IR) and far infrared (FIR) radiances measured from orbit with extremely high absolute
accuracy are a critical observation for future climate benchmark missions. For the infrared radiance spectra, it has been
determined that a measurement accuracy, expressed as an equivalent brightness temperature error, of 0.1 K (k = 3)
confirmed on orbit is required for signal detection above natural variability for decadal climate signatures [1, 2].
The challenge in the sensor development for a climate benchmark measurement mission is to achieve ultra-high
accuracy with a design that can be flight qualified, has long design life, and is reasonably small, simple, and affordable.
The required simplicity is achievable due to the large differences in the sampling and noise requirements for the
benchmark climate measurement from those of the typical remote sensing infrared sounders for weather research or
operational weather prediction.
The University of Wisconsin Space Science and Engineering Center, with funding from the NASA Instrument Incubator
Program (IIP), developed the Absolute Radiance Interferometer (ARI), which is designed to meet the uncertainty
requirements needed to establish spectrally resolved thermal infrared climate benchmark measurements from space. The
ARI is a prototype instrument designed to have a short upgrade path to a spaceflight instrument.
Recent vacuum testing of the ARI, conducted under funding from the NASA Earth Science Technology Office, has
demonstrated the capability to meet the 0.1 K (k = 3) uncertainty requirement on-orbit. An overview of the instrument
design and summary of the radiometric performance verification of the UW-SSEC ARI will be presented.
The Atmospheric Chemistry Experiment (ACE) is a mission on-board the Canadian Space Agency’s (CSA) SCISAT-1. ACE is composed of a suite of instruments consisting of an infrared Fourier Transform Spectrometer (FTS) coupled with an auxiliary imager monitoring aerosols based on the extinction of solar radiation using two filtered detectors (visible and near infrared). A suntracker is also included to provide fine pointing during occultation. A second instrument, MAESTRO, is a spectrophotometer covering the near ultra-violet to the near infrared. In combination, the instrument payload covers the spectral range from 0.25 to 13.3 μm. The ACE mission came about from a need to better understand the chemical and dynamical processes that control the distribution of ozone in the upper troposphere and stratosphere, with particular emphasis on the Arctic region. Measurement of the vertical distribution of molecular species in these portions of the atmosphere permits elucidation of the key chemical and dynamical processes. The ACE-FTS measures the vertical distributions of trace gases as well as polar stratospheric clouds, aerosols, and temperature by a solar occultation technique from low earth orbit. By measuring solar radiation at high spectral resolution as it passes through different layers of the atmosphere, the absorption thus measured provides information on vertical profiles of atmospheric constituents, temperature, and pressure. Detailed and sensitive vertical distribution of trace gases help to better understand the chemical processes not only for ozone formation and destruction but also for other dynamic processes in the atmosphere. The ACE/SCISAT-1 satellite was successfully launched by NASA on August 12, 2003, and has been successfully operating since, now celebrating its 10th year on-orbit anniversary. This paper presents a summary of the heritage and development history of the ACE-FTS instrument. Design challenges and solutions are related. The actual on-orbit performance is presented, and the health status of the instrument payload is discussed. Potential future follow-on missions are finally introduced.
The PCW (Polar Communications and Weather) mission is a dual satellite mission with each satellite in a highly eccentric orbit with apogee ~42,000 km and a period (to be decided) in the 12–24 hour range to deliver continuous communications and meteorological data over the Arctic and environs. Such as satellite duo can give 24×7 coverage over the Arctic. The operational meteorological instrument is a 21-channel spectral imager similar to the Advanced Baseline Imager (ABI). The PHEOS-WCA (weather, climate and air quality) mission is intended as an atmospheric science complement to the operational PCW mission. The target PHEOS-WCA instrument package considered optimal to meet the full suite of science team objectives consists of FTS and UVS imaging sounders with viewing range of ~4.5° or a Field of Regard (FoR) ~ 3400×3400 km2 from near apogee. The goal for the spatial resolution at apogee of each imaging sounder is 10×10 km2 or better and the goal for the image repeat time is targeted at ~2 hours or better. The FTS has 4 bands that span the MIR and NIR with a spectral resolution of 0.25 cm−1. They should provide vertical tropospheric profiles of temperature and water vapour in addition to partial columns of many other gases of interest for air quality. The two NIR bands target columns of CO2, CH4 and aerosol optical depth (OD). The UVS is an imaging spectrometer that covers the spectral range of 280–650 nm with 0.9 nm resolution and targets the tropospheric column densities of O3 and NO2 and several other Air Quality (AQ) gases as well the Aerosol Index (AI).
Spectrally resolved infrared (IR) and far infrared (FIR) radiances measured from orbit with extremely high absolute
accuracy (< 0.1 K, k = 3, brightness temperature at scene temperature) constitute a critical observation for future climate
benchmark missions.
The challenge in the IR/FIR Fourier Transform Spectrometer (FTS) sensor development for a climate benchmark
measurement mission is to achieve the required ultra-high accuracy with a design that can be flight qualified, has long
design life, and is reasonably small, simple, and affordable. In this area, our approach is to make use of components
with strong spaceflight heritage (direct analogs with high TRL) combined into a functional package for detailed
performance testing. The required simplicity is achievable due to the large differences in the sampling and noise
requirements for the benchmark climate measurement from those of the typical remote sensing infrared sounders for
weather research or operations.
A summary of the instrument design and development, and the radiometric performance of the Absolute Radiance
Interferometer (ARI) at the University of Wisconsin Space Science and Engineering Center (UW-SSEC) will be
presented.
A summary of the development of the Absolute Radiance Interferometer (ARI) at the University of Wisconsin Space
Science and Engineering Center (UW-SSEC) will be presented. At the heart of the sensor is the ABB CLARREO
Interferometer Test-Bed (CITB), based directly on the ABB Generic Flight Interferometer (GFI). This effort is funded
under the NASA Instrument Incubator Program (IIP).
KEYWORDS: Signal to noise ratio, Sensors, Mirrors, Space operations, Fourier transforms, NOx, Infrared spectroscopy, Imaging systems, Signal detection, Satellites
The Atmospheric Chemistry Experiment (ACE) is the mission on-board Canadian Space Agency's science satellite,
SCISAT-1. ACE consists of a suite of instruments in which the primary element is an infrared Fourier Transform
Spectrometer (FTS) coupled with an auxiliary 2-channel visible (525 nm) and near infrared imager (1020 nm). A
secondary instrument, a grating spectrometer named MAESTRO, provides spectrographic data from the near ultra-violet
to the near infrared, including the visible spectral range. With all instruments combined, the payload covers the spectral
range from 0.25 to 13.3 micron. A comprehensive set of simultaneous measurements of trace gases, thin clouds, aerosols
and temperature are being made by solar occultation from this satellite in low earth orbit. The ACE mission measures
and analyses the chemical and dynamical processes that control the distribution of ozone in the upper troposphere and
stratosphere. A high inclination (74°), low earth orbit (650 km) allows coverage of tropical, mid-latitude and polar
regions. The ACE/SciSat-1 spacecraft was launched by NASA on August 12th, 2003.
This paper presents the status of the ACE-FTS instrument, after nearly five years on-orbit. On-orbit SNR and some
telemetry signals are presented. The health status of the instrument is discussed.
The Atmospheric Chemistry Experiment (ACE) is the mission on-board Canadian Space Agency's science satellite,
SCISAT-1. ACE consists of a suite of instruments in which the primary element is an infrared Fourier Transform
Spectrometer (FTS) coupled with an auxiliary 2-channel visible (525 nm) and near infrared imager (1020 nm). A
secondary instrument, MAESTRO, provides spectrographic data from the near ultra-violet to the near infrared, including
the visible spectral range. In combination, the instrument payload covers the spectral range from 0.25 to 13.3 micron. A
comprehensive set of simultaneous measurements of trace gases, thin clouds, aerosols and temperature are being made
by solar occultation from this satellite in low earth orbit. The ACE mission measures and analyses the chemical and
dynamical processes that control the distribution of ozone in the upper troposphere and stratosphere. A high inclination
(740), low earth orbit (650 km) allows coverage of tropical, mid-latitude and polar regions. The ACE/SciSat-1 spacecraft
was launched by NASA on August 12th, 2003.
This paper presents the status of the ACE-FTS instrument, after four years on-orbit. On-orbit performance is presented.
The health and safety status of the instrument payload is discussed. Optimization of on-orbit performance is presented as
well as operational aspects. Aspects related to reliability of FTS are discussed as well as potential future follow-on
missions.
The Atmospheric Chemistry Experiment (ACE) is the mission on-board Canadian Space Agency's science satellite, SCISAT-1. ACE consists of a suite of instruments in which the primary element is an infrared Fourier Transform Spectrometer (FTS) coupled with an auxiliary 2-channel visible (525 nm) and near infrared imager (1020 nm). A secondary instrument, MAESTRO, provides spectrographic data from the near ultra-violet to the near infrared, including the visible spectral range. In combination, the instrument payload covers the spectral range from 0.25 to 13.3 micron. A comprehensive set of simultaneous measurements of trace gases, thin clouds, aerosols and temperature are being made by solar occultation from this satellite in low earth orbit. The ACE mission measures and analyses the chemical and dynamical processes that control the distribution of ozone in the upper troposphere and stratosphere. A high inclination (74°), low earth orbit (650 km) allows coverage of tropical, mid-latitude and polar regions. The ACE/SciSat-1 spacecraft was launched by NASA on August 12th, 2003. This paper presents the status of the ACE-FTS instrument, after three years on-orbit. On-orbit performances as well as their optimization are presented. Needs for future missions similar to ACE are discussed.
KEYWORDS: Signal to noise ratio, Fourier transforms, Imaging systems, Transmittance, Sensors, Mirrors, Sun, Space operations, Visible radiation, Near infrared
The Atmospheric Chemistry Experiment (ACE) is the mission selected by the Canadian Space Agency (CSA) for its science satellite, SCISAT-1. ACE consists of a suite of instruments in which the primary element is an infrared Fourier Transform Spectrometer (FTS) coupled with an auxiliary 2-channel visible (525 nm) and near infrared imager (1020 nm). A secondary instrument, MAESTRO, provides spectrographic data from the near ultra-violet to the near infrared, including the visible spectral range. In combination the instrument payload covers the spectral range from 0.25 to 13.3 micron. A comprehensive set of simultaneous measurements of trace gases, thin clouds, aerosols and temperature are made by solar occultation from a satellite in low earth orbit. The ACE mission measures and analyses the chemical and dynamical processes that control the distribution of ozone in the upper troposphere and stratosphere. A high inclination (74 degrees), low earth orbit (650 km) allows coverage of tropical, mid-latitude and polar regions. The ACE/SciSat-1 spacecraft was launched by NASA on August 12th, 2003.
This paper presents the on-orbit performance of the ACE-FTS instrument. The commissioning activities allowed the activation of the various elements of the instrument and the optimization of several parameters such as gains, integration times, pointing offsets, etc. The performance validation was the last phase of the instrument hardware commissioning activities. The results of the performance validation are presented in terms of on-orbit instrument performance with respect to instrument requirements such as signal-to-noise ratio, transmittance accuracy, and spectral resolution. Results are also compared to ground validation tests performed during the thermal-vacuum campaigns. Performance is presented in terms of validation of instrument from an engineering perspective.
Both Fourier Transform Infrared (FTIR) spectrometers and sampling techniques have seen a paradigm shift over the past 20 years. Infrared (IR) spectroscopy using the mid IR “fingerprint” region shows excellent specificity for determining the presence and quantity of well over 50000 organic chemical species. Tiny amounts of sample suffice for identification using a chemically inert scratch resistant diamond micro internal reflection crystal. For air quality, FTIR
can be used as a point monitor, sniffing air samples in an IR cell or using a long open-air path with a remote reflector or direct passive remote sensing. This makes IR ideal for first responders and haz/mat professionals provided the FTIR is compact, rugged and easy to use in the field. Already FTIR is widely used in industrial plants often directly at the process. In parallel FTIR is increasingly used in mobile field environments including airborne platforms as well as for
satellite-based sounders. This paper presents a resume of the evolution of FTIR and sampling technology and the boundaries of applicability of field deployed FTIR chemical sensors for the assessment of suspect substances as well as air pollution at the site of an emergency situation.
Near the start of activity in FT-IR, the most important feature was sensitivity as derived from the multiplex and throughput advantages. It permitted weak emission, very high resolution spectroscopy and later the exploitation of such techniques as diffuse reflectance and photoacoustic spectroscopy in the mid IR region. Carefully configured FT-IR systems in well controlled laboratory environments provide excellent reproducibility. This permitted extension to IR spectroscopy where small changes in large signals could be measured. Even today reproducibility is frequently demonstrated as a measure of FT-IR performance via the well known 100% line. Of course in the use of quantitative analysis methods sensitivity and reproducibility are of importance, but they are by no means a complete specification of the performance of an FT-IR based analyzer using a chemometric method.
The present work was performed in order to extend the study of the relative intensities of lines within the isotope structure to other spectral transitions of different symmetry, especially of B1 yields E symmetry, and to study in more detail the widths and shapes of lines due to impurity centers with different lithium isotope composition, using the better resolution of a diode laser spectrometer (1 (DOT) 10-4 cm-1), all this being important for quantitative isotopic composition analyses.
The cryogenic interferometer is an optimized sensor for low level infrared spectral measurements. An ideal application is emissivity measurements of low-temperature samples, since room temperature spectrometers become background limited by instrument self-emission in such cases. For a cryogenic instrument, operation near background limited performance for targets at 220 K with emissivity of 0.05 is possible by cooling the complete instrument to around 77 K. This instrument has been designed for operation in the laboratory, and most of the parameters are remote controlled by the data processing PC. Spectral resolution is variable from 4 cm-1 to 128 cm-1. The spectral range covered is from 600 cm-1 to 4000 cm-1. The system is built into an Infrared Lab Cryostat, providing a holding time of 48 hours. This instrument is the second cryogenic spectrometer built by Bomem, the first being the balloon-borne SIRIS, a high resolution system for atmospheric research.
KEYWORDS: Calibration, Black bodies, Signal to noise ratio, Spectrometers, Temperature metrology, Spectral calibration, Aerospace engineering, FT-IR spectroscopy, Fourier transforms, Liquids
FTIR instruments aimed at low temperature emission measurements require a two-point radiometric calibration because of significant emission from the instrument itself. Calibration measurements with two reference blackbodies are conducted for ground instruments. In space, the low temperature reference blackbody can be substituted with deep space observation. On the ground, pointing at a liquid nitrogen bath is used. Calibration operations involve complex arithmetics to obtain from reference and actual scene measurements a calibrated spectrum. Frequency and duration of calibration measurements are dependent upon instrument stability and noise budgets. When reference spectra are free of high resolution features, calibration measurements can be performed at a resolution lower than that of actual scene measurements. The Michelson interferometer for passive atmospheric sounding (MIPAS) will limb sound the atmosphere by measuring its mid-infrared emission with an apodized resolution of 0.05 cm-1. This instrument is used as an example to illustrate the trade-offs required in calibrating an emission FTIR. Given the current expected temperature variations of the instrument over the orbit, MIPAS will require a deep space reference measurement after every altitude scan, and a combined deep space and blackbody measurement at a lower frequency. For an adequate acquisition efficiency, low resolution calibration measurements are performed, at 0.2 cm-1 or 1 cm(superscript -1.
Semiconductor materials are used for the fabrication of devices for electronic and optical applications. Optical characterization techniques are among the most powerful methods to assess the general quality of semiconductor crystals. The optical methods can determine impurity content as well as assessing crystal morphology. They can also be used to study other properties of newly created materials. In practical terms they are non-destructive and simple to perform (no contacts required). Optical characterization methods monitor electronic transitions, local vibrational modes and other processes inside the material studied. The photons associated with these transitions carry very precise information about energy levels of the pure material and those induced by the presence of the impurities. These assaying methods can be classified under two general categories, according to the way the optical signature is supplied. Emission-type measurements include photoluminescence and Raman spectroscopy while absorption-type measurements include IR absorption, photocurrent and photothermal ionization spectroscopy (PTIS).
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